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Deep-Seated Gravitational Slope Deformation Scaling on Mars And Earth Surf. Dynam. Discuss., https://doi.org/10.5194/esurf-2018-27 Manuscript under review for journal Earth Surf. Dynam. Discussion started: 4 April 2018 c Author(s) 2018. CC BY 4.0 License. Deep-seated gravitational slope deformation scaling on Mars and Earth: same fate for different initial conditions and structural evolutions Olga Kromuszczyńska1, Daniel Mège2,3,4, Krzysztof Dębniak1, Joanna Gurgurewicz1,2, Magdalena 5 Makowska1 and Antoine Lucas5 1Institute of Geological Sciences, Polish Academy of Sciences, Research Centre in Wrocław, Podwale 75, 50-449 Wrocław, Poland 2Space Research Centre, Polish Academy of Sciences, Bartycka 18A, 00-716 Warsaw, Poland 10 3Laboratoire de Planétologie et Géodynamique, Université de Nantes, UMR CNRS 6112, 2 rue de la houssinière, Nantes, France 4Observatoire des Sciences de l'Univers Nantes Atlantique, OSUNA CNRS UMS 3281, Nantes, France 5Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris, Diderot, Paris 75013, France Correspondence to: Daniel Mège ([email protected]) 15 Abstract. Some of the most spectacular instances of deep-seated gravitational slope deformation (DSGSD) are found on Mars in the Valles Marineris region. They provide an excellent opportunity to study DSGSD phenomenology using a scaling approach. The topography of selected DSGSD scarps in Valles Marineris and in the Tatra Mountains is investigated after their likely similar postglacial origin is established. The deformed Martian ridges are larger than the deformed terrestrial ridges by one to two orders, with however a similar height-to-width ratio, ~0.24. The measured finite strain of the Valles Marineris 20 ridges is 3 times larger than in the Tatra Mountains, suggesting that starting from two different initial conditions, with steeper slopes in Valles Marineris, the final ridge geometry is now similar. Because DSGSD is expected to be now inactive in both regions, their comparison suggests that whatever the initial ridge morphology, DSGSD proceeds until a mature profile is attained. On both planets, strain is distributed over the same number (~5) of major scarps; fault displacements are therefore much larger on Mars. The large offsets make necessary reactivation of the DSGSD fault scarps in Valles Marineris, whereas 25 single seismic events would be enough to generate DSGSD fault scarps in the Tatra Mountains. The required longer activity of the Martian faults may be correlated with a long succession of climate cycles generated by the unstable Mars obliquity. In spite of similar global geometry today, the studied ridges on Mars and Earth affected by DSGSD did not start from similar initial conditions and did not follow the same structural evolution. 1 Earth Surf. Dynam. Discuss., https://doi.org/10.5194/esurf-2018-27 Manuscript under review for journal Earth Surf. Dynam. Discussion started: 4 April 2018 c Author(s) 2018. CC BY 4.0 License. 1 Introduction 1.1 The dissected Valles Marineris hillslopes The Valles Marineris bedrock hillslopes show a dissected, "spur-and-gully" morphology at a glance similar to the morphology of alpine mountains, locally degraded at the first order into tributary canyons and huge landslides (Lucchitta, 1978; Patton, 5 1991; Lucchitta et al., 1992). Spur-and-gully dissection has taken the form of subparallel, digitate spurs separated by gullies covered by long slope deposits (Lucchitta, 1978; Howard, 1989). The upper parts of the slopes are steeper than the lower parts (Lucchitta, 1978). The latter are covered by talus of material accumulated at the angle-of-repose (Patton, 1981). The spurs are usually perpendicular to the slope; however, in some areas, their oblique orientation relative to chasma trend suggests structural control by vertical fractures oblique to the troughs that must be tens of kilometres long (Sharp 1973; Blasius et al., 1977). 10 High resolution image data available since the early 2000's have revealed that outside these tributary canyons and huge landslides, the dissected, pristine morphology shows a variety of smaller-scale geomorphological features which are familiar to mountain geomorphologists, with the association or superimposition of a rich variety of landforms controlled by mountain permafrost degradation, streams erosion, talus development, and gravity (Mège and Bourgeois, 2011; Gourronc et al., 2014; Dębniak et al., 2017). The difference with alpine mountain geomorphology on Earth is therefore not that much a matter of 15 morphological details; it rather lies in the size of the landsystems. In the main troughs, the height of the Valles Marineris slopes is several kilometres, and up to 10 km, whereas typical mountain slopes on Earth are hundreds to a few kilometres high. 1.2 Deep-seated gravitational slope deformation in Valles Marineris This work focuses on a series of morphotectonic features observed along Valles Marineris walls displaying the spur-and-gully morphology, including uphill-facing normal faults scarps and crestal grabens. Such features are systematically observed when 20 spur-and-gully dissection occurs on internal ridges within the main Valles Marineris chasmata. They denote extensional tectonics, but boundary forces that result in crustal “rifting” are unlikely to be the cause of this deformation even though rifting is frequently considered to have been a major contributor to the formation of some of the main Valles Marineris chasmata (e.g., Masson, 1977; Frey, 1979; Schultz, 1991, 1995a, 1998; Mège and Masson, 1996a, 1996b; Peulvast et al., 2001; Mège et al., 2017). One of the main reasons is that uphill-facing scarps and crestal grabens have not been reported to have formed in 25 terrestrial rift zones on Earth nor are they expected to form in experimental models (e.g., Corti, 2012 for the East African Rift System). In extreme cases, when crustal stretching has been on the order of hundreds of percent, cracking and normal faulting is pervasive in horsts as much as in grabens (Angelier and Colletta; 1983), which has certainly not been the case in Valles Marineris (e.g. Schultz 1991, 1995a; Mège and Masson 1996b; Mège et al. 2003). Another reason is that when the basal ridge slope topography can be accurately studied (i.e. not mantled by debris aprons), 30 normal faulting on the ridge crest and slopes appears to be counterbalanced by basal slope bulging (Mège and Bourgeois, 2011). Ridge-top splitting has been interpreted by Lucchitta et al. (1992) and Treiman (2008) as crustal zones strengthened by dyke intrusion or cemented by central fractures. Arguing that such a fracture origin is not well documented on Earth either, 2 Earth Surf. Dynam. Discuss., https://doi.org/10.5194/esurf-2018-27 Manuscript under review for journal Earth Surf. Dynam. Discussion started: 4 April 2018 c Author(s) 2018. CC BY 4.0 License. Mège and Bourgeois (2011), Kromuszczyńska et al. (2012) and Gourronc et al. (2014) interpreted these features as an effect of deep-seated gravitational slope deformation (DSGSD). Uphill-facing normal faulting and crestal extensional deformation is indeed well documented on Earth in areas of DSGSD (review in Mège and Bourgeois, 2011). In most described terrestrial instances, such as in the Alps of Europe, Japan and New Zealand, the Andes and others, where DSGSD has been described in 5 mountain ridges glaciated during the Quaternary (review in Mège and Bourgeois, 2011), Such a postglacial context, in the Valles Marineris case, is adapted to the recently identified and widespread glacial landsystem (Gourronc et al., 2014; Mège et al., 2017; Dębniak et al., 2017), is also in agreement with expected slope deformation in this context (Makowska et al., 2016), and additionally provides a good framework to understand the detected mineralogical occurrences as from CRISM (Mège and Bourgeois, 2011; Cull et al., 2014). Postglacial deformation, as far as DSGSD is concerned, includes the paraglacial response 10 of rock slopes to changing stress conditions after glacier retreat, (e.g., Ballantyne, 2002), i.e. hillslope debuttressing, but also some longer term deformation made possible or facilitated by slope debuttressing. This includes upslope migration of stress release, and postglacial water flow, pressure variations and subcritical failure occurring for instance within the framework of the geologic response to climate cyclicity (Pánek et al., 2017). In this work, we will therefore assume that DSGSD is the most likely origin for the uphill-facing scarps and crestal grabens 15 observed on the slopes of the Valles Marineris spur-and-gully ridges. We also consider that a postglacial origin is likely, given its consistency and adaptation to the evidence of a widespread Valles Marineris glacial landsystem subject to short-period climatic variations (Laskar et al., 2004; Levrard et al., 2004) under which additional slope morphologies may develop (e.g., Quantin et al. 2005; Chojnacki et al., 2016). 1.3 Scaling of processes involved in deep-seated gravitational slope deformation 20 Some gravity processes do not similarly develop at different scales. For instance, landslide propagation does not depend on fully similar parameters when small and large. Landslides that are small with respect to mountain size are influenced by the surrounding mountainous topography, the first effect of which being the development of an inclined transport channel that overlies an accumulation of debris on a less inclined slope. An example is the Thurwieser landslide in the central Alps (e.g., Sosio et al., 2008). For landslides that involve a large
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